We began with the times of primary eclipse obtained from the ten half-sector eclipse light curves. The errorbars from the Monte Carlo analysis were significantly too small so we multiplied them by a factor of 20 to better account for their scatter versus a fitted linear ephemeris. To these we added published times of primary minimum obtained using CCDs or photoelectric photometers, plus the zeropoint of the orbital ephemeris given by Mallama [1]}. These values were in all cases quoted in HJD, so we converted them to BJD. When a time system was given it was always UTC, so we assumed that all published timings were on the UTC system and converted them to TDB to match those from TESS, using routines from Eastman et al. [2]}.
